BAYESIAN MASS ESTIMATES OF THE MILKY WAY: THE DARK AND LIGHT SIDES OF PARAMETER ASSUMPTIONS

We present mass and mass profile estimates for the Milky Way (MW) Galaxy using the Bayesian analysis developed by Eadie et al. and using globular clusters (GCs) as tracers of the Galactic potential. The dark matter and GCs are assumed to follow different spatial distributions; we assume power-law model profiles and use the model distribution functions described in Evans et al. and Deason et al. We explore the relationships between assumptions about model parameters and how these assumptions affect mass profile estimates. We also explore how using subsamples of the GC population beyond certain radii affect mass estimates. After exploring the posterior distributions of different parameter assumption scenarios, we conclude that a conservative estimate of the Galaxy's mass within 125 kpc is 5.22 x 10(11) M-circle dot, with a 50% probability region of (4.79, 5.63) x 10(11) M-circle dot. Extrapolating out to the virial radius, we obtain a virial mass for the MW of 6.82 x 10(11) M-circle dot with 50% credible region of (6.06, 7.53) x 10(11) M-circle dot(r(vir) = 185(-7)(+7) kpc). If we consider only the GCs beyond 10 kpc, then the virial mass is 9.02(5.69, 10.86) x 10(11) M-circle dot (r(vir) 198(-24)(+19) kpc). We also arrive at an estimate of the velocity anisotropy parameter beta of the GC population, which is beta = 0.28 with a 50% credible region (0.21, 0.35). Interestingly, the mass estimates are sensitive to both the dark matter halo potential and visible matter tracer parameters, but are not very sensitive to the anisotropy parameter.